Merger of black hole-neutron star binaries: nonspinning black hole case

Masaru Shibata; Koji Uryu

doi:10.1103/PhysRevD.74.121503

paper

Merger of black hole-neutron star binaries: nonspinning black hole case

arXiv:gr-qc/0612142 · doi:10.1103/PhysRevD.74.121503

Abstract

We perform a simulation for merger of a black hole (BH)-neutron star (NS) binary in full general relativity preparing a quasicircular state as initial condition. The BH is modeled by a moving puncture with no spin and the NS by the $Γ$ -law equation of state with $Γ = 2$ . Corotating velocity field is assumed for the NS. The mass of the BH and the rest-mass of the NS are chosen to be $\approx 3.2 M_{⊙}$ and $\approx 1.4 M_{⊙}$ with relatively large radius of the NS $\approx 14$ km. The NS is tidally disrupted near the innermost stable orbit but $\sim 80$ of the material is swallowed into the BH with small disk mass $\sim 0.3 M_{⊙}$ even for such small BH mass $\sim 3 M_{⊙}$ . The result indicates that the system of a BH and a massive disk of $\sim M_{⊙}$ is not formed from nonspinning BH-NS binaries, although a disk of mass $\sim 0.1 M_{⊙}$ is a possible outcome.

5 pages. Phys. Rev. D 74, 121503 (R) (2006)

Merger of black hole-neutron star binaries: nonspinning black hole case

Abstract

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